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Chemical Abundances in the Universe: Connecting First Stars to Planets

Proceedings IAU Symposium No. 265, 2009 K. Cunha, M. Spite & B. Barbuy, eds.

c

 International Astronomical Union 2010 doi:10.1017/S1743921310001171

Light elements in stars with exoplanets

E. Delgado Mena

1

, M. C. G´

alvez-Ortiz

2

, J. I. Gonz´

alez-Hern´

andez

3

,

G. Israelian

1

, N.C. Santos

4

,

5

, R. Rebolo

1

,

6

and C. Dominguez

Cerde˜

na

1

1

Instituto de Astrof´ısica de Canarias, E-38200 La Laguna, Tenerife, Spain. email: edm@iac.es

2Centre for Astrophysics Research, Science and Technology Research Institute, University of

Hertfordshire, Hatfield AL10 9AB, UK.

3

Departamento de Astrof´ısica, Facultad de Ciencias F´ısicas, Universidad Complutense de Madrid, E-28040, Spain.

4

Centro de Astrof´ısica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal.

5Observatoire de Gen`eve, 51 ch. des Maillettes, CH-1290 Sauverny, Switzerland. 6

Consejo Superior de Investigaciones Cient´ıficas, E-28006, Madrid, Spain.

Abstract. Light elements are important tracers of the internal stellar structure and kinematics.

Li and Be are both burned in the stellar interiors but Be requires much higher temperatures and thus we can expect to measure Be abundances in stars which have no detectable Li in their atmospheres. The study of these elements can give us information about processes related to the angular momentum history of these stars, since rotation and angular momentum loss are important mechanisms responsible for the depletion of light elements. Additionally, if pollution has played an important role in determining the high-metal content of planet host stars, we would expect to find a similar or even higher increase in the Li and Be contents. We present Be and Li abundances in a sample of 69 stars with planets and 31 stars without known planetary companion, spanning a large range of effective temperatures.

Keywords. stars: abudances, stars: fundamental parameters, stars: planetary systems, stars:

planetary systems: formation, stars: atmospheres

In Fig. 1 we present the derived Be abundances as a function of effective tempera-ture. Be shows a trend similar to previous works if we exclude the subgiant stars with temperatures below 4900 K. Overall, no clear difference seems to exist between planet hosts and comparison stars. Be abundances decrease from a maximum near Teff = 6100 K towards both higher and lower temperatures although there is an object that does not follow this trend. Very little, if any, depletion has occurred for stars of this effec-tive temperature. A similar maximum for the Li abundances is also found at about the same temperature. For higher temperatures the values of log N(Be) decrease forming the well-known Be gap for F stars, a feature that has a counterpart for Li. The maximum at 6100 K may be attributed to Galactic chemical evolution effects, since most of the stars in the temperature interval between 6000 and 6200 K are particularly metal-rich, and Galactic Be abundances are known to increase with the metallicity (Rebolo et al. 1988, Boesgaard et al. 1999). However, high Be abundances are not observed in low tempera-ture metal-rich stars. The fact that Be abundances decrease at low temperatempera-tures can be seen as evidence that Be is burned during the main sequence evolution of these stars but this low abundances are not predicted by models (Pinsonneault et al. 1990).

Be and Li abundances are shown in the right panel of Fig. 1. This figure tells us that overall, and taking into account only dwarfs, there seems to be a correlation between the depletions of Li and Be, in the sense that stars that have depleted their Be have also

430

at https:/www.cambridge.org/core/terms. https://doi.org/10.1017/S1743921310001171

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Light elements in stars with exoplanets 431

Figure 1. Left panel: Beryllium abundances as a function of effective temperature for stars

with (open stars) and without (filled circles) known planets from Santos et al. (2002, 2004) andalvez Ortiz et al. (2009, submitted). Abundances below log N(Be)∼ 0.8 are not predicted by models (Pinsonneault et al. 1990) at Te f f < 5500 K. Right panel: Beryllium abundances as a

function of lithium bundances for stars with (red symbols) and without (black symbols) known planets from G´alvez Ortiz et al. (2009, submitted).

strongly depleted their Li. We can see that objects with temperatures above 6000 K are situated in the upper right corner where there is a maximum of Li and Be values. In the temperature regime between 5600 and 6000 K a large dispersion in the Li abundances is observed while Be remains close to the primordial value. Stars with temperatures below 5600 K are mostly situated in the left upper-middle panel where both Li and Be are clearly depleted. This temperature seems to mark the onset of strong Be depletion while severe Li depletion begins at 5900 K.

The results presented for Be can be explained in terms of the Galactic chemical evolu-tion. A comparison of the Be abundances of planet hosts and ’single’ stars has revealed that, perhaps with a few exceptions, the two samples follow the same behaviour in the log N(Be) vs. Tef f plot. Nevertheless, we have found a small group of stars that present

particularly high Be abundances that could signal pollution effects, although other ex-planations are possible. Measurements of 6Li/7Li ratio will allow to find signatures of planetary accretion.

References

Boesgaard, A. M., Deliyannis, C. P., King, J. R. et al. 1999, AJ, 117, 1549 Fischer, D. A. & Valenti, J. 2005, ApJ, 622, 1102

alvez-Ortiz, M.C., Delgado Mena, E., Santos, N.C., Israelian, G. et al. 2009, A&A, submitted Israelian, G., Santos, N. C., Mayor, M., & Rebolo, R. 2003, A&A, 405, 753

Israelian, G., Santos, N. C., Mayor, M., & Rebolo, R. 2004, A&A, 414, 601

Kurucz, R. L. 1993, CD-ROMs, ATLAS9 Stellar Atmospheres Programs (Cambridge:

Smithso-nian Astrophys. Obs.)

Pinsonneault, M. H., Kawaler, S. D., & Demarque, P. 1990, ApJS, 74, 501 Rebolo, R., Abia, C., Beckman, J. E., & Molaro, P. 1988, A&A, 193, 193

Santos, N. C., Garca Lpez, R. J., Israelian, G., Mayor, M., Rebolo, R., Garca-Gil, A., Prez de Taoro, M. R., & Randich, S. 2002, A&A, 386, 1028

Santos, N. C., Israelian, G., Randich, S., Garca Lpez, R. J., & Rebolo, R. 2004, A&A, 425, 1013 Santos, N. C., Israelian, G., Garca Lpez, R. J., Mayor, M., Rebolo, R., Randich, S., Ecuvillon,

A., & Domnguez Cerdea, C. 2004, A&A, 427, 1085

Sousa, S. G., Santos, N. C., Mayor, M., Udry, S., Casagrande, L., Israelian, G., Pepe, F., Queloz, D., Monteiro, M. J. P. F. G. 2008, A&A, 487, 373

at https:/www.cambridge.org/core/terms. https://doi.org/10.1017/S1743921310001171

Figure

Figure 1. Left panel: Beryllium abundances as a function of effective temperature for stars with (open stars) and without (filled circles) known planets from Santos et al

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